Abstract
Observations are presented of emission line resonance polarization in Fe xiii λ10747 at the total solar eclipse of 12 November 1966. Useful data, with angular resolution 15″, describe three quadrants of the corona from 1.08 R ⊙ to a maximum of 1.6 R ⊙. The direction of the electric vector of observed polarization is perpendicular to the solar limb, to the limits of accuracy of measurement, in at least 74% of all cases. Departures in the other points are consistent with the magnetic depolarization expected from the non-radial fields of streamers. Polarizations observed range from near zero at the limb to 80 % and higher at 1.6 R ⊙. Averaged polarization is highest in non-streamer regions, where above 1.2 R ⊙ it suggests pure radiative excitation of the λ10747 line. Below 1.2 R ⊙, and in a dense streamer, the polarization is significantly depressed, indicating dominant collisional excitation of the line wherever the electron density exceeds 50 × 106 cm−3.
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The National Center for Atmospheric Research is sponsored by the National Science Foundation.
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Eddy, J.A., Lee, R.H. & Emerson, J.P. The λ 747 coronal line at the 1966 eclipse. Sol Phys 30, 351–369 (1973). https://doi.org/10.1007/BF00152667
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DOI: https://doi.org/10.1007/BF00152667